Neptune trojan

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Neptune's L4 trojans with plutinos for reference. .mw-parser-output .legend{page-break-inside:avoid;break-inside:avoid-column}.mw-parser-output .legend-color{display:inline-block;min-width:1.25em;height:1.25em;line-height:1.25;margin:1px 0;text-align:center;border:1px solid black;background-color:transparent;color:black}.mw-parser-output .legend-text{} Neptune trojans (selection) * 2001 QR322 * 2005 TN53 * 2007 VL305 Plutinos * Pluto * Orcus * Ixion NTrojans Plutinos 55AU.svg
Neptune's L4 trojans with plutinos for reference.
  Neptune trojans (selection)
  · 2001 QR322
  · 2005 TN53
  · 2007 VL305 		   Plutinos
  · Pluto
  · Orcus
  · Ixion

Neptune trojans are bodies that orbit the Sun near one of the stable Lagrangian points of Neptune, similar to the trojans of other planets. They therefore have approximately the same orbital period as Neptune and follow roughly the same orbital path. Thirty-one Neptune trojans are currently known, of which 27 orbit near the Sun–Neptune L4 Lagrangian point 60° ahead of Neptune [1] and four orbit near Neptune's L5 region 60° behind Neptune. [1] The Neptune trojans are termed 'trojans' by analogy with the Jupiter trojans.

Contents

The discovery of 2005 TN53 in a high-inclination (>25°) orbit was significant, because it suggested a "thick" cloud of trojans [2] (Jupiter trojans have inclinations up to 40° [3] ), which is indicative of freeze-in capture instead of in situ or collisional formation. [2] It is suspected that large (radius ≈ 100 km) Neptune trojans could outnumber Jupiter trojans by an order of magnitude. [4] [5]

In 2010, the discovery of the first known L5 Neptune trojan, 2008 LC18 , was announced. [6] Neptune's trailing L5 region is currently very difficult to observe because it is along the line of sight to the center of the Milky Way, an area of the sky crowded with stars.

Discovery and exploration

In 2001, the first Neptune trojan was discovered, (612243) 2001 QR322 , near Neptune's L4 region, and with it the fifth [a] known populated stable reservoir of small bodies in the Solar System. In 2005, the discovery of the high-inclination trojan 2005 TN53 has indicated that the Neptune trojans populate thick clouds, which has constrained their possible origins (see below).

On August 12, 2010, the first L5 trojan, 2008 LC18 , was announced. [6] It was discovered by a dedicated survey that scanned regions where the light from the stars near the Galactic Center is obscured by dust clouds. [7] This suggests that large L5 trojans are as common as large L4 trojans, to within uncertainty, [7] further constraining models about their origins (see below).

It would have been possible for the New Horizons spacecraft to investigate L5 Neptune trojans discovered by 2014, when it passed through this region of space en route to Pluto. [5] Some of the patches where the light from the Galactic Center is obscured by dust clouds are along New Horizons's flight path, allowing detection of objects that the spacecraft could image. [7] 2011 HM102 , the highest-inclination Neptune trojan known, was just bright enough for New Horizons to observe it in end-2013 at a distance of 1.2 AU. [8] However, New Horizons may not have had sufficient downlink bandwidth, so it was eventually decided to give precedence to the preparations for the Pluto flyby. [9] [10]

Dynamics and origin

An animation showing the path of six of Neptune's L4 trojans in a rotating frame with a period equal to Neptune's orbital period. Neptune is held stationary. (Click to view.) Neptunian Trojans.gif
An animation showing the path of six of Neptune's L4 trojans in a rotating frame with a period equal to Neptune's orbital period. Neptune is held stationary. (Click to view.)

The orbits of Neptune trojans are highly stable; Neptune may have retained up to 50% of the original post-migration trojan population over the age of the Solar System. [2] Neptune's L5 can host stable trojans equally well as its L4. [11] Neptune trojans can librate up to 30° from their associated Lagrangian points with a 10,000-year period. [7] Neptune trojans that escape enter orbits similar to centaurs. [11] Although Neptune cannot currently capture stable trojans, [2] roughly 2.8% of the centaurs within 34 AU are predicted to be Neptune co-orbitals. Of these, 54% would be in horseshoe orbits, 10% would be quasi-satellites, and 36% would be trojans (evenly split between the L4 and L5 groups). [12]

The unexpected high-inclination trojans are the key to understanding the origin and evolution of the population as a whole. [11] The existence of high-inclination Neptune trojans points to a capture during planetary migration instead of in situ or collisional formation. [2] [7] The estimated equal number of large L5 and L4 trojans indicates that there was no gas drag during capture and points to a common capture mechanism for both L4 and L5 trojans. [7] The capture of Neptune trojans during a migration of the planets occurs via process similar to the chaotic capture of Jupiter trojans in the Nice model. When Uranus and Neptune are near but not in a mean-motion resonance the locations where Uranus passes Neptune can circulate with a period that is in resonance with the libration periods of Neptune trojans. This results in repeated perturbations that increase the libration of existing trojans causing their orbits to become unstable. [13] This process is reversible allowing new trojans to be captured when the planetary migration continues. [14] For high-inclination trojans to be captured the migration must have been slow, [15] or their inclinations must have been acquired previously. [16]

Colors

The first four discovered Neptune trojans have similar colors. [2] They are modestly red, slightly redder than the gray Kuiper belt objects, but not as extremely red as the high-perihelion cold classical Kuiper belt objects. [2] This is similar to the colors of the blue lobe of the centaur color distribution, the Jupiter trojans, the irregular satellites of the gas giants, and possibly the comets, which is consistent with a similar origin of these populations of small Solar System bodies. [2]

The Neptune trojans are too faint to efficiently observe spectroscopically with current technology, which means that a large variety of surface compositions are compatible with the observed colors. [2]

Several Neptunian Trojans have been observed to have very-red colors similar to cold classical Kuiper belt objects. [17]

Naming

In 2015, the IAU adopted a new naming scheme for Neptune trojans, which are to be named after Amazons, with no differentiation between objects in L4 and L5. [18] The Amazons were an all-female warrior tribe that fought in the Trojan War on the side of the Trojans against the Greeks. As of 2019, the named Neptune trojans are 385571 Otrera (after Otrera, the first Amazonian queen in Greek mythology) and 385695 Clete (after Clete, an Amazon and the attendant to the Amazons' queen Penthesilea, who led the Amazons in the Trojan war). [19] [20]

Members

The amount of high-inclination objects in such a small sample, in which relatively fewer high-inclination Neptune trojans are known due to observational biases, [2] implies that high-inclination trojans may significantly outnumber low-inclination trojans. [11] The ratio of high- to low-inclination Neptune trojans is estimated to be about 4:1. [2] Assuming albedos of 0.05, there are an expected 400+250
−200 Neptune trojans with radii above 40 km in Neptune's L4. [2] This would indicate that large Neptune trojans are 5 to 20 times more abundant than Jupiter trojans, depending on their albedos. [2] There may be relatively fewer smaller Neptune trojans, which could be because these fragment more readily. [2] Large L5 trojans are estimated to be as common as large L4 trojans. [7]

(612243) 2001 QR322 and 2008 LC18 display significant dynamical instability. [11] This means they could have been captured after planetary migration, but may as well be a long-term member that happens not to be perfectly dynamically stable. [11]

As of September 2023, 31 Neptune trojans are known, of which 27 orbit near the Sun–Neptune L4 Lagrangian point 60° ahead of Neptune, [1] 4 orbit near Neptune's L5 region 60° behind Neptune, and one orbits on the opposite side of Neptune (L3) but frequently changes location relative to Neptune to L4 and L5. [1] These are listed in the following table. It is constructed from the list of Neptune trojans maintained by the IAU Minor Planet Center [1] and with diameters from Sheppard and Trujillo's paper on 2008 LC18 , [7] unless otherwise noted.

Name Prov.
designation 		Lagrangian
point 		q ( AU ) Q ( AU ) e i (°) Abs. mag Diameter [b]
(km)		Year of
identification		Notes MPC
(316179) 2010 EN65 L3 21.10940.6130.31019.27.2~2202010Jumping trojan MPC
385571 Otrera 2004 UP10 L4 29.31830.9420.0311.48.8~1002004First Neptune trojan numbered and named MPC
385695 Clete 2005 TO74 L4 28.46931.7710.0525.38.3~1302005– MPC
(527604) 2007 VL305 L4 28.13032.0280.06528.18.5~1202007– MPC
(530664) 2011 SO277 L4 29.62230.5030.0099.67.8~1702016– MPC
(530930) 2011 WG157 L4 29.06430.8780.02522.37.3~2102016– MPC
(612243) 2001 QR322 L4 29.40431.0110.0311.38.1~1402001First Neptune trojan discovered, unstable Trojan
(613490) 2006 RJ103 L4 29.07731.0140.0288.27.6~1802006– MPC
2004 KV18 L5 24.55335.8510.18313.68.71102011Temporary Neptune trojan MPC
2005 TN53 L4 28.09232.1620.06725.09.0~902005First high-inclination trojan discovered [2] MPC
2008 LC18 L5 27.36532.4790.07927.68.2~1302008First L5 trojan discovered [7] MPC
(666739) 2010 TS191 L4 28.60831.2530.0486.68.1~1402016– MPC
2010 TT191 L4 27.91332.1890.0704.37.8~1602016– MPC
2011 HM102 L5 27.66232.4550.08329.48.1~1302012– MPC
2012 UV177 L4 27.80632.2590.07220.89.3~80 [21] 2014– MPC
2012 UD185 L4 28.79431.5380.04228.47.6~1802019– MPC
2013 KY18 L5 26.62434.0840.1246.66.8~2602016Stability uncertain MPC
2013 RL124 L4 29.36630.7830.02810.18.8~1002020– MPC
2013 RC158 L4 28.61131.7840.0537.58.9~1002021– MPC
2013 TZ187 L4 28.09232.1350.06613.18.2~1402020– MPC
2013 TK227 L4 27.78732.6830.08118.69.6~702021– MPC
2013 VX30 L4 27.56332.5250.08731.38.3~1302018– MPC
2014 QO441 L4 26.96133.2150.10118.88.3~130 [21] 2014Most eccentric stable Neptune trojan [22] MPC
2014 QP441 L4 28.13731.9710.06719.49.3~802015– MPC
2014 RO74 L4 28.42631.6140.05029.58.4~1202020– MPC
2014 SC374 L4 27.03833.0600.09633.78.2~1402020– MPC
2014 UU240 L4 28.66131.4570.04535.88.2~1402018– MPC
2014 YB92 L4 27.30933.2430.09830.88.6~1102021– MPC
2015 RW277 L4 27.74232.2360.07430.810.2~502018– MPC
2015 VV165 L4 27.51332.4970.08616.99.0~902018– MPC
2015 VW165 L4 28.48831.4880.0495.08.4~1202018– MPC
2015 VX165 L4 27.61232.3270.07317.29.2~902018– MPC
2015 VU207 L4 29.21131.1740.03338.97.3~2102021Highest known inclination MPC

(613100) 2005 TN74 [23] and (309239) 2007 RW10 [24] were thought to be Neptune trojans at the time of their discovery, but further observations have disconfirmed their membership. 2005 TN74 is currently thought to be in a 3:5 resonance with Neptune. [25] (309239) 2007 RW10 is currently following a quasi-satellite loop around Neptune. [26]

See also

Notes

  1. ↑ After the asteroid belt, the Jupiter trojans, the trans-Neptunian objects and the Mars trojans.
  2. ↑ assuming an albedo of 0.05

Related Research Articles

<span class="mw-page-title-main">Jupiter trojan</span> Asteroid sharing the orbit of Jupiter

The Jupiter trojans, commonly called trojan asteroids or simply trojans, are a large group of asteroids that share the planet Jupiter's orbit around the Sun. Relative to Jupiter, each trojan librates around one of Jupiter's stable Lagrange points: either L4, existing 60° ahead of the planet in its orbit, or L5, 60° behind. Jupiter trojans are distributed in two elongated, curved regions around these Lagrangian points with an average semi-major axis of about 5.2 AU.

<span class="mw-page-title-main">Hilda asteroid</span> Group of asteroids in orbital resonance with Jupiter

The Hilda asteroids are a dynamical group of more than 6,000 asteroids located beyond the asteroid belt but within Jupiter's orbit, in a 3:2 orbital resonance with Jupiter. The namesake is the asteroid 153 Hilda.

<span class="nowrap">(612243) 2001 QR<sub>322</sub></span>

(612243) 2001 QR322, prov. designation: 2001 QR322, is a minor planet and the first Neptune trojan discovered, by American astronomer Marc Buie of the Deep Ecliptic Survey at Cerro Tololo Observatory in Chile on 21 August 2001. It orbits ahead of Neptune at its L4 Lagrangian point and measures approximately 132 kilometers (82 miles) in diameter.

In astronomy, a resonant trans-Neptunian object is a trans-Neptunian object (TNO) in mean-motion orbital resonance with Neptune. The orbital periods of the resonant objects are in a simple integer relations with the period of Neptune, e.g. 1:2, 2:3, etc. Resonant TNOs can be either part of the main Kuiper belt population, or the more distant scattered disc population.

<span class="mw-page-title-main">Scattered disc</span> Collection of bodies in the extreme Solar System

The scattered disc (or scattered disk) is a distant circumstellar disc in the Solar System that is sparsely populated by icy small Solar System bodies, which are a subset of the broader family of trans-Neptunian objects. The scattered-disc objects (SDOs) have orbital eccentricities ranging as high as 0.8, inclinations as high as 40°, and perihelia greater than 30 astronomical units (4.5×109 km; 2.8×109 mi). These extreme orbits are thought to be the result of gravitational "scattering" by the gas giants, and the objects continue to be subject to perturbation by the planet Neptune.

2005 TN53 is an inclined Neptune trojan leading Neptune's orbit in the outer Solar System, approximately 80 kilometers in diameter. It was first observed on 7 October 2005, by American astronomers Scott Sheppard and Chad Trujillo at Las Campanas Observatory in the Atacama desert of Chile. It was the third such body to be discovered, and the first with a significant orbital inclination, which showed that the population as a whole is very dynamically excited.

385695 Clete, provisional designation 2005 TO74, is a Neptune trojan, co-orbital with the ice giant Neptune, approximately 97 kilometers (60 miles) in diameter. It was named after Clete, one of the Amazons from Greek mythology. The minor planet was discovered on 8 October 2005, by American astronomers Scott Sheppard and Chad Trujillo at Las Campanas Observatory in Chile. 23 known Neptune trojans have already been discovered.

<span class="mw-page-title-main">Irregular moon</span> Captured satellite following an irregular orbit

In astronomy, an irregular moon, irregular satellite, or irregular natural satellite is a natural satellite following a distant, inclined, and often highly elliptical and retrograde orbit. They have been captured by their parent planet, unlike regular satellites, which formed in orbit around them. Irregular moons have a stable orbit, unlike temporary satellites which often have similarly irregular orbits but will eventually depart. The term does not refer to shape; Triton, for example, is a round moon but is considered irregular due to its orbit and origins.

<span class="mw-page-title-main">Trojan (celestial body)</span> Objects sharing the orbit of a larger one

In astronomy, a trojan is a small celestial body (mostly asteroids) that shares the orbit of a larger body, remaining in a stable orbit approximately 60° ahead of or behind the main body near one of its Lagrangian points L4 and L5. Trojans can share the orbits of planets or of large moons.

In astronomy, a co-orbital configuration is a configuration of two or more astronomical objects orbiting at the same, or very similar, distance from their primary; i.e., they are in a 1:1 mean-motion resonance..

<span class="mw-page-title-main">Mars trojan</span> Celestial bodies that share the orbit of Mars

The Mars trojans are a group of trojan objects that share the orbit of the planet Mars around the Sun. They can be found around the two Lagrangian points 60° ahead of and behind Mars. The origin of the Mars trojans is not well understood. One theory suggests that they were primordial objects left over from the formation of Mars that were captured in its Lagrangian points as the Solar System was forming. However, spectral studies of the Mars trojans indicate this may not be the case. Another explanation involves asteroids chaotically wandering into the Mars Lagrangian points later in the Solar System's formation. This is also questionable considering the short dynamical lifetimes of these objects. The spectra of Eureka and two other Mars trojans indicates an olivine-rich composition. Since olivine-rich objects are rare in the asteroid belt it has been suggested that some of the Mars trojans are captured debris from a large orbit-altering impact on Mars when it encountered a planetary embryo.

<span class="mw-page-title-main">Nice model</span> Scenario for the dynamical evolution of the Solar System

In astronomy, the Nicemodel is a scenario for the dynamical evolution of the Solar System. It is named for the location of the Côte d'Azur Observatory—where it was initially developed in 2005—in Nice, France. It proposes the migration of the giant planets from an initial compact configuration into their present positions, long after the dissipation of the initial protoplanetary disk. In this way, it differs from earlier models of the Solar System's formation. This planetary migration is used in dynamical simulations of the Solar System to explain historical events including the Late Heavy Bombardment of the inner Solar System, the formation of the Oort cloud, and the existence of populations of small Solar System bodies such as the Kuiper belt, the Neptune and Jupiter trojans, and the numerous resonant trans-Neptunian objects dominated by Neptune.

2008 LC18 is a Neptune trojan first observed on 7 June 2008 by American astronomers Scott Sheppard and Chad Trujillo using the Subaru Telescope at Mauna Kea Observatories on Hawaii, United States. It was the first object found in Neptune's trailing L5 Lagrangian point and measures approximately 100 kilometers in diameter.

2004 KV18 is an eccentric Neptune trojan trailing Neptune's orbit in the outer Solar System, approximately 70 kilometers in diameter. It was first observed on 24 May 2004, by astronomers at the Mauna Kea Observatories on Hawaii, United States. It was the eighth Neptune trojan identified and the second in Neptune's L5 Lagrangian point.

The five-planet Nice model is a numerical model of the early Solar System that is a revised variation of the Nice model. It begins with five giant planets, the four that exist today plus an additional ice giant between Saturn and Uranus in a chain of mean-motion resonances.

<span class="nowrap">(316179) 2010 EN<sub>65</sub></span>

(316179) 2010 EN65 is a trans-Neptunian object orbiting the Sun. However, with a semi-major axis of 30.8 AU, the object is actually a jumping Neptune trojan, co-orbital with Neptune, as the giant planet has a similar semi-major axis of 30.1 AU. The body is jumping from the Lagrangian point L4 into L5 via L3. As of 2016, it is 54 AU from Neptune. By 2070, it will be 69 AU from Neptune.

<span class="nowrap">(687170) 2011 QF<sub>99</sub></span>

(687170) 2011 QF99 is a minor planet from the outer Solar System and the first known Uranus trojan to be discovered. It measures approximately 60 kilometers (37 miles) in diameter, assuming an albedo of 0.05. It was first observed 29 August 2011 during a deep survey of trans-Neptunian objects conducted with the Canada–France–Hawaii Telescope, but its identification as Uranian trojan was not announced until 2013.

The jumping-Jupiter scenario specifies an evolution of giant-planet migration described by the Nice model, in which an ice giant is scattered inward by Saturn and outward by Jupiter, causing their semi-major axes to jump, and thereby quickly separating their orbits. The jumping-Jupiter scenario was proposed by Ramon Brasser, Alessandro Morbidelli, Rodney Gomes, Kleomenis Tsiganis, and Harold Levison after their studies revealed that the smooth divergent migration of Jupiter and Saturn resulted in an inner Solar System significantly different from the current Solar System. During this migration secular resonances swept through the inner Solar System exciting the orbits of the terrestrial planets and the asteroids, leaving the planets' orbits too eccentric, and the asteroid belt with too many high-inclination objects. The jumps in the semi-major axes of Jupiter and Saturn described in the jumping-Jupiter scenario can allow these resonances to quickly cross the inner Solar System without altering orbits excessively, although the terrestrial planets remain sensitive to its passage.

<span class="mw-page-title-main">Extreme trans-Neptunian object</span> Solar system objects beyond the other known trans-Neptunian objects

An extreme trans-Neptunian object (ETNO) is a trans-Neptunian object orbiting the Sun well beyond Neptune (30 AU) in the outermost region of the Solar System. An ETNO has a large semi-major axis of at least 150–250 AU. The orbits of ETNOs are much less affected by the known giant planets than all other known trans-Neptunian objects. They may, however, be influenced by gravitational interactions with a hypothetical Planet Nine, shepherding these objects into similar types of orbits. The known ETNOs exhibit a highly statistically significant asymmetry between the distributions of object pairs with small ascending and descending nodal distances that might be indicative of a response to external perturbations.

12929 Periboea, provisional designation: 1999 TZ1, is a dark Jupiter trojan from the Trojan camp, approximately 54 kilometers (34 miles) in diameter. It was discovered on 2 October 1999, by American astronomer Charles W. Juels at the Fountain Hills Observatory in Arizona. Originally considered a centaur, this now re-classified Jovian asteroid has a rotation period of 9.3 hours and belongs to the 80 largest Jupiter trojans. It was named from Greek mythology after Periboea, mother of Pelagon by the river-god Axius.

References

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  13. ↑ Kortenkamp, Stephen J.; Malhotra, Renu; Michtchenko, Tatiana (2004). "Survival of Trojan-type companions of Neptune during primordial planet migration". Icarus. 167 (2): 347–359. arXiv: astro-ph/0305572 . Bibcode:2004Icar..167..347K. doi:10.1016/j.icarus.2003.09.021. S2CID   2046901.
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  20. ↑ "385695 Clete (2005 TO74)". Minor Planet Center. 18 May 2019. Retrieved 10 June 2019.
  21. 1 2 "Conversion of Absolute Magnitude to Diameter". www.physics.sfasu.edu. Archived from the original on 23 March 2010. Retrieved 29 April 2018.
  22. ↑ Gerdes, D. W.; Jennings, R. J.; Bernstein, G. M.; Sako, M.; Adams, F.; Goldstein, D.; Kessler, R.; Abbott, T.; Abdalla, F. B.; Allam, S.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Capozzi, D.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.; DePoy, D. L.; Desai, S.; Dietrich, J. P.; Doel, P.; Eifler, T. F.; Neto, A. Fausti; Flaugher, B.; Frieman, J.; Gaztanaga, E.; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Honscheid, K.; James, D. J.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Li, T. S.; Maia, M. A. G.; March, M.; Martini, P.; Miller, C. J.; Miquel, R.; Nichol, R. C.; Nord, B.; Ogando, R.; Plazas, A. A.; Romer, A. K.; Roodman, A.; Sanchez, E.; Santiago, B.; Schubnell, M.; Sevilla-Noarbe, I.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Suchyta, E.; Swanson, M. E. C.; Tarlé, G.; Thaler, J.; Walker, A. R.; Wester, W.; Zhang, Y. (28 January 2016). "Observation of Two New L4 Neptune Trojans in the Dark Energy Survey Supernova Fields". The Astronomical Journal. 151 (2): 39. arXiv: 1507.05177 . Bibcode:2016AJ....151...39G. doi: 10.3847/0004-6256/151/2/39 . S2CID   55326461.
  23. ↑ MPEC 2005-U97 : 2005 TN74, 2005 TO74 Minor Planet Center
  24. ↑ "Distant EKOs, 55". Archived from the original on 2013-05-25. Retrieved 2012-07-24.
  25. ↑ "Orbit and Astrometry for 05TN74". www.boulder.swri.edu. Archived from the original on 29 April 2018. Retrieved 29 April 2018.
  26. ↑ de la Fuente Marcos; de la Fuente Marcos (2012). "(309239) 2007 RW10: a large temporary quasi-satellite of Neptune". Astronomy and Astrophysics Letters. 545: L9. arXiv: 1209.1577 . Bibcode:2012A&A...545L...9D. doi:10.1051/0004-6361/201219931. S2CID   118374080.
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